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Table 8:

Different setups for different mass-metallicity relations found in the literature, and associated shifts to be applied to their stellar masses in order for them to be comparable with our results. This table shows the type of data, the models, the presence or not of secondary bursts, and the IMF used to compute the stellar masses. The last column gives the global shift that has to be applied to the logarithm of the stellar mass.

References $^{\dagger}$
Data$^{\star}$ Model Bursts IMF $^{\dagger}$ Sum
our study P+S CB07 yes C03  
T04 S BC03 yes K01  
  +0.00 -0.07 - -0.056 -0.126
S05 P Pégase yes BG03  
  +0.05 -0.09 - +0.024 -0.016
E06 P BC03 no C03  
  +0.05 -0.09 +0.14 - +0.1
M08 P BC03 no S55  
  +0.05 -0.09 +0.14 -0.232 -0.132
$^{\star}$ S stands for spectroscopy, P stands for photometry. $^{\dagger}$ T04: Tremonti et al. (2004); S05: Savaglio et al. (2005); E06: Erb et al. (2006); M08: Maiolino et al. (2008); C03: Chabrier (2003); K01: Kroupa (2001); BG03: Baldry & Glazebrook (2003); S55: Salpeter (1955).

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